New Views of the UniverseNew Views of the UniverseNew Views of the UniverseNew Views of the Universe

Rocky Kolb (don’t call me Mike Turner)Rocky Kolb (don’t call me Mike Turner)Particle Astrophysics Center, Fermilab & University ChicagoParticle Astrophysics Center, Fermilab & University Chicago

David Schramm’s LegacyDavid Schramm’s Legacy

Jerry WasserburgThe Lunartic Asylum

Willy FowlerKellogg Radiation Laboratory

Dave’s Ph. D. advisors at Caltech

Some of Willy’s Boys

Dave Arnett, Jean Audoze, John Bahcall, Dick Bond,

Geoff Burbidge, Margaret Burbidge, Don Clayton,

George Fuller, Rocky Kolb, Grant Matthews,

Dave Schramm, Gary Steigman, Jim Truran,

Bob Wagoner, Craig Wheeler, Stan Woosley, …

Precision cosmologyPrecision cosmologyPrecision cosmologyPrecision cosmology

MAPWMAPGreater accuracy if combine with other data

• CMB• 2dFGRS• SDSS• Ly-• SN Ia• Consult entrails of chickens,• prophecies of Nostradamus,• & the Kabbalah

Priors

CDMCDMCDMCDM

• Inflation-produced perturbations• Baryo/leptogenesis

Mission accomplished …Mission accomplished …Mission accomplished …Mission accomplished …

… … or premature jubilation?or premature jubilation?… … or premature jubilation?or premature jubilation?

How Far Will They Go?How Far Will They Go?

Desperate

PhysicistsDesperate

Physicists

How Far Will They Go?How Far Will They Go?Inflation • Dark Energy • Dark Matter

V() • • SUSY

Dark-matterDark-matterDark-matterDark-matter

dynamics x-ray gaslensing

MatterMatterM M

MatterMatterM M

power spectrum

cmb simulations

QSO 1937-1009

Ly

Burles et al.Tytler

BaryonsBaryonsB B BaryonsBaryonsB B agrees with WMAP

Bn n

freeze out

actual

equilibrium

X

T/MX

1010

Rel

ativ

e ab

un

dan

ce

1510

2010

510

010

1 2 31 10 10 10

/e M T

Cold thermal relicsCold thermal relicsCold thermal relicsCold thermal relics

• s-wave or p-wave?• annihilation or scattering cross section?• co-annihilation?• sub-leading dependence on mass, g*, etc.• targets are nuclei (spin-dependence)

Not quite so clean:

X / a

Cold thermal relics Cold thermal relics X X AACold thermal relics Cold thermal relics X X AA

X A

X X q q

X

X

q

q

X S

X q X q

X

q q

X

X P

q q X X Xq

q X

Seeking SUSYSeeking SUSYSeeking SUSYSeeking SUSYHierarchy problem:• fundamental scale is Planck mass*• observe particles with mass much less than Planck mass

o gauge bosons protected by gauge symmetryo fermions protected by chiral symmetryo scalars (e.g., Higgs) defenseless!

• introduce supersymmetry to protect scalars

Supersymmetric Standard Model: 105 parameters

Constrained Minimal Supersymmetric Standard Model: 3 parameters:

Lightest supersymmetric particle (LSP) stable: neutralino?

1/ 2 0tan , , , sign( )m m

* Assumed here to be 1/ 2NG

• Direct detection (S)

More than a dozen experiments

• Indirect detection (A)

Annihilation in sun, Earth, galaxy. . .

neutrinos, positrons,

antiprotons, rays, . . .

• Accelerator production (P)

Tevatron, LHC, ILC

Cold thermal relics (neutralino)Cold thermal relics (neutralino)Cold thermal relics (neutralino)Cold thermal relics (neutralino)

• SUSY shaded areas

• Probing significant regions of MSSM model space

• Light-mass region largely ruled out

• Another factor of 100 may be needed Combined

Soudan limits

DAMA NaI/1-4 3region

ZEPLIN I

EDELWEISS

Cryogenic Dark Matter Search

Cold thermal relicsCold thermal relicsCold thermal relicsCold thermal relics

Muons from the sunMuons from the sunMuons from the sunMuons from the sun

“For every complex natural phenomenon there is a simple, elegant, compelling,wrong explanation.”

- Tommy Gold

The nature of dark matter is a complex natural phenomenon.

The neutralino is a simple, elegant, compelling explanation.

Many variations of errorMany variations of errorMany variations of errorMany variations of error

• neutrinos (hot dark matter)

• sterile neutrinos, gravitinos (warm dark matter)

• axions, axion clusters

• LKP (lightest Kaluza-Klein particle)

• supermassive wimpzillas

• solitons (Q-balls; B-balls; Odd-balls, Screw-balls….)

• LSP (neutralino, axino, …) (cold dark matter)

axions

axion clusters

6 40

8 25

10 eV (10 g)

10 M (10 g)

Mass range

Noninteracting: wimpzillas

Strongly interacting: B balls

Interaction strength range

InflationInflationInflationInflation

( )V

?Who is the inflaton

InflationBig Bang plus 10-35? seconds

Big Bang plus 380,000 Years

Big Bang plus 14 Billion Years

Seeds of Structure+

Gravitational Waves

Imprint of inflationImprint of inflationImprint of inflationImprint of inflation

1. a (nearly exact) power-law

2. spectrum of gaussian

3. super-Hubble-radius

4. scalar perturbations (seeds of structure) &

5. tensor perturbations (gravitational waves)

6. related by a consistency relation

7. in their growing mode

8. in a spatially flat universe.

Comparison to observation:Comparison to observation:Comparison to observation:Comparison to observation:

Harrison-Zel’dovichHarrison-Zel’dovichSpectrum ?Spectrum ?

Harrison-Zel’dovichHarrison-Zel’dovichSpectrum ?Spectrum ?

n=1?, n’=0?, r=0?

• Combine CMB, LSS, Ly-?• Tensor modes?• Consistency relation?

1. Who is the inflaton?

• models of inflation, reconstruction?

2. Transplanckian physics?

• probe of short-distance physics?

3. Defrosting?

• preheating, reheating, ….?

4. Extra dimensions, brane, bulk, etc.?

• new dynamics?

5. Other particle production?

• WIMPZILLAS, gravitnos, ….?

6. Are perturbations from the inflaton fluctuations?

• curvaton, modulon, …

IssuesIssuesIssuesIssues

“For every complex natural phenomenon there is a simple, elegant, compelling, butwrong explanation.”

- Tommy Gold

The nature of inflation is a complex natural phenomenon.

Single-field, slow-roll inflation is a simple, elegant, compelling explanation.

The gravity of dark energyThe gravity of dark energyThe gravity of dark energyThe gravity of dark energy

Main Entry: grav·i·ty   Function: nounEtymology: Middle French or Latin; Middle French gravité, from Latin gravitat-, gravitas, from gravis

1 a : dignity or sobriety of bearing b : IMPORTANCE, SIGNIFICANCE; especially : SERIOUSNESS c : a serious situation or problem2 : WEIGHT3 a (1) : the gravitational attraction of the mass of the earth, the moon, or a planet for bodies at or near its surface (2) : a fundamental physical force that is responsible for interactions which occur because of

3) age of the universe

4) structure formation

5)

2) subtractionTOTAL = 0.3

The case for :1) Hubble diagram dL(z)

MATTER

V

AC

UU

M

Einstein-de Sitterflat, matter-dominated model(maximum theoretical bliss)

Illogical magnitude (what’s it related to?):

4 430 -3 4 310 g cm 10 eV 10 cm

Cosmo-illogical constant?Cosmo-illogical constant?Cosmo-illogical constant?Cosmo-illogical constant?

2 229 338 10 cm 10 eVG

Illogical timing (why now?):

BBNEWKGUT

M R

REC

• eV scalar fields!!!• modification of gravity• extra dimensions• branes and bulk• Lorentz violating vector fields• Friedmann equation incomplete• • • • (then there are the crazy ideas)

anthropic principle(the landscape)

scalar fields

Practical tools for dark energyPractical tools for dark energyPractical tools for dark energyPractical tools for dark energy

Now entertain conjecture of a timeWhen creeping murmur and the poring darkFills the wide vessel of the universe. — King Henry Vth

Entertaining conjectureEntertaining conjectureEntertaining conjectureEntertaining conjecture

(creeping murmur)(creeping murmur)

Modifying the left-hand sideModifying the left-hand sideModifying the left-hand sideModifying the left-hand side• Braneworld modifies Friedmann equation

• Phenomenological approach

• Gravitational force law modified at large distance

• Tired gravitons

• Gravity repulsive at distance R Gpc

• n=1 KK graviton mode very light, m (Gpc)

• Einstein & Hilbert got it wrong

• Backreaction of inhomogeneities

Freese & Lewis 12

cutoff1n

H A

Five-dimensional at cosmic distances

Deffayet, Dvali& Gabadadze

Gravitons metastable - leak into bulkGregory, Rubakov & Sibiryakov;

Dvali, Gabadadze & Porrati

Kogan, Mouslopoulos, Papazoglou, Ross & Santiago

Csaki, Erlich, Hollowood & Terning

Räsänen; Kolb, Matarrese, Notari & Riotto;Notari; Kolb, Matarrese & Riotto

Binetruy, Deffayet, Langlois

1 4 416S G d x g R R Carroll, Duvvuri, Turner, Trodden

Acceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneities

• Most conservative approach — nothing new – no new fields (like eV mass scalars)– no extra long-range forces– no modification of general relativity– no modification of Newtonian gravity at large distances– no Lorentz violation– no extra dimensions, bulks, branes, etc.– no faith-based (anthropic) reasoning

• Magnitude?: calculable from observables related to

• Why now?: acceleration triggered by era of non-linear structure

Acceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneitiesHomogeneous model Inhomogeneous model

3

h

h h

h h h

V a

H a a

3

i

i i

i i i

x

V a

H a a

h i x

We (Kolb, Matarrese, Riotto + others) think not!

?h iH H

Acceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneitiesAcceleration from inhomogeneities• View scale factor as zero-momentum mode of gravitational field

• In homogeneous/isotropic model it is the only degree of freedom

• Inhomogeneities: non-zero modes of gravitational field

• Non-zero modes interact with and modify zero-momentum mode

cosmology scalar-field theory

zero-mode a hi (vev of a scalar field)

non-zero modes inhomogeneities thermal/finite-density bkgd.

modify a(t) modify h(t)i e.g., acceleration e.g., phase transitions

Cosmology scalar field theory analogue

physical effect

Different approachesDifferent approachesDifferent approachesDifferent approaches

• Expansion rate of an

inhomogeneous Universe expansion rate of homogeneous Universe with hi

• Inhomogeneities modify zero-mode [effective scale

factor is aD VD]

• Effective scale factor has a (global) effect on observables

• Potentially can account for acceleration without dark energy or modified GR

• Model an inhomogeneous Universe as a homogeneous Universe model with hi

• Zero mode [a(t) / V] is the zero mode of a homogeneous model with hi

• Inhomogeneities only have a local effect on observables

• Cannot account for observed acceleration

Standard approach Our approach

DON’T KILL

ROCKY

Acceleration without dark energy!!!!!Acceleration without dark energy!!!!!Acceleration without dark energy!!!!!Acceleration without dark energy!!!!!

• Hirata• Fry• Afshordi

This meeting:Many issues:• non-perturbative nature• shell crossing• comparison to observed LSS• gauge/frame choices• physical meaning of coarse graining

Program:

• can inhomogeneities change effective zero mode?• how does (does it?) affect observables?• can one design an inhomogeneous universe that accelerates?• could it lead to an apparent dark energy?• can it be reached via evolution from usual initial conditions?• does it at all resemble our universe?• large perturbative terms resum to something harmless?

H(z)

dL(z) dA(z) V(z)

baryonosc.

stronglensing

CMBweak

lensingSNIA clusters

clustercounting

Growth of structure

CMBcluster

countingweak

lensingP(k,z)

How Do We Sort It Out?How Do We Sort It Out?How Do We Sort It Out?How Do We Sort It Out?Precision measurements of w, wa,

Test gravity

solar systemmillimeter

scaleaccelerators P(k,z)

Galileo Galilei Cosimo II

++++

Medicean stars

William Herschel George III

++++

Georgium sidus

Dark energy parameter, Dark energy parameter, wwDark energy parameter, Dark energy parameter, ww

w ++++

George “Dubya” Bush

George II

New Views of the UniverseNew Views of the UniverseNew Views of the UniverseNew Views of the Universe

Rocky Kolb Particle Astrophysics Center, FermilabRocky Kolb Particle Astrophysics Center, Fermilab& University of Chicago& University of Chicago

David Schramm’s LegacyDavid Schramm’s Legacy